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We present the first results from MMT and Keck spectroscopy for a largesample of $0.1\leq z\leq1$ emission-line galaxies selected from our narrow-bandimaging in the Subaru Deep Field. We measured the weak [OIII]$\lambda$4363emission line for 164 galaxies (66 with at least 3$\sigma$ detections, and 98with significant upper limits). The strength of this line is set by theelectron temperature for the ionized gas. Because the gas temperature isregulated by the metal content, the gas-phase oxygen abundance is inverselycorrelated with [OIII]$\lambda$4363 line strength. Our temperature-basedmetallicity study is the first to span $\approx$8 Gyr of cosmic time and$\approx$3 dex in stellar mass for low-mass galaxies, $\log{\left(M_{\rmstar}/M_{\rm sun}\right)}\approx6.0-9.0$. Using extensive multi-wavelengthphotometry, we measure the evolution of the stellar mass--gas metallicityrelation and its dependence on dust-corrected star formation rate (SFR). Thelatter is obtained from high signal-to-noise Balmer emission-line measurements.Our mass-metallicity relation is consistent with Andrews & Martini at$z\leq0.3$, and evolves toward lower abundances at a given stellar mass,$\log{({\rm O/H})}\propto(1+z)^{-2.32^{+0.52}_{-0.26}}$. We find that galaxieswith lower metallicities have higher SFRs at a given stellar mass and redshift,although the scatter is large ($\approx$0.3 dex), and the trend is weaker thanseen in local studies. We also compare our mass--metallicity relation againstpredictions from high-resolution galaxy formation simulations, and find goodagreement with models that adopt energy- and momentum-driven stellar feedback.We have identified 16 extremely metal-poor galaxies with abundances less than atenth of solar; our most metal-poor galaxy at $z\approx0.84$ is similar to I Zw18.

astrophysical journal/the astrophysical journal

The Metal Abundances across Cosmic Time ($\mathcal{MACT}$) Survey. II.  Evolution of the Mass-Metallicity Relation over 8 Billion Years, using  [OIII]$\lambda$4363\AA-based Metallicities